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QUIET Summary

QUIET Summary. Probing Inflationary Scalar fields at GUT-scale energies Phase I has already demonstrated its technology and methodology (100 detectors) The most sensitive CMB polarization array yet fielded Phase II has been proposed NSF Reverse site visit in Jan-Feb

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QUIET Summary

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  1. QUIET Summary • Probing Inflationary Scalar fields at GUT-scale energies • Phase I has already demonstrated its technology and methodology (100 detectors) • The most sensitive CMB polarization array yet fielded • Phase II has been proposed • NSF Reverse site visit in Jan-Feb • FNAL involvement critical to get to Phase II level (1600) • “HEP” approach more important as experiments grow • QUIET is unique: (verified) technology, frequencies, year-round access, best able to forecast sensitivity, and alliances with other experiments • The Cosmic Microwave Background and Particle Physics • M. Kamionkowski, A. Kosowsky, Ann.Rev.Nucl.Part.Sci.49:77-123,1999 • The Cosmic Microwave Background for Pedestrians: A Review for Particle and Nuclear Physicists • D. Samtleben, S. Staggs, B. W., Ann.Rev.Nucl.Part.Sci.57:245-283,2007

  2. Manchester Oxford Chicago (KICP) Fermilab Oslo MPI-Bonn Stanford (KIPAC) KEK Caltech JPL Columbia Princeton Miami Chajnantor Plateau, Chile FNAL PAC 2

  3. The Site: Atacama Desert in Chile • Home for many expts • ALMA, ACT, ASTE, QUIET, POLARBEAR, CLOVER, … • High and Dry: • 16,700 feet • Year-round access • Lots of room FNAL PAC

  4. FNAL PAC

  5. Integrating the W-band Array the Chicago (5 times as many elements to be integrated at FNAL) FNAL PAC

  6. Ey Ea Eb Ex 4kHz phase switching Q U QUIET L/R Correlator: Simultaneous Q/U measurements FNAL PAC An Unpolarized pixel gives ZERO even with a gain difference between the legs!

  7. 8 sec of data 100kHz sampling Temperature vs. time, 10 ms bins unswitched switched FNAL PAC

  8. Map precision on 1x1 degree pixel: Planck: 1 K (100 GHz) QUIET: 10-1K (90 GHz) FNAL PAC

  9. Q U Galaxy (Pol., <100 hrs) sytematicefects not considered yet WMAP 5 years FNAL PAC

  10. QUIET CMB Temperature Map(1 detector, 1 month vs. 5 years) FNAL PAC

  11. QUIET ~ 600 hrs WMAP 5 years QUIET-I Stokes Q map of one patch: Already deeper than Planck forecasts FNAL PAC

  12. Null Power Spectra FNAL PAC

  13. Phase I has already shown: • Platelet, OMT technology works • Module technology works • Want to improve sensitivity and production • Crossed Dragone Optics verified • Now the most popular choice • High speed sampling works and is valuable • The site works: duty cycle, atmosphere • We can reliable forecast Phase II • Cautious approach has paid off FNAL PAC

  14. QUIET Phase-I Forecasts FNAL PAC

  15. Phase II Plan • 4 Telescopes • (3 CMB & 1 Foreground) • “Small things” • Electronics improvements • Thermal control • Matching band-passes • “Big things” • Improving module production • Improving module performance FNAL PAC

  16. QUIET Polarbear ABS, SPT Foregrounds(Planck Sky Model) • Dust(synchrotron) negligible for QUIET(SPT) • Broad frequency range important to determine contamination • 100% overlap with ABS, Polarbear; less w/SPT r=0.1 FNAL PAC

  17. Current* Performance (noise, duty cycle, 1/f) Likely Improvements 0.018r0.005  FNAL PAC < 0.3 ev 10lensing35 * already better!

  18. “While QUIET I has been pursued primarily with non-HEP funding, HEP has unique capabilities to offer the project as it moves to the next step, QUIET II: (a) Fermilab has unique large-scale fabrication capabilities required to mass-produce the detectors; (b) HEP scientists have valuable experience with the high-speed electronics the project will require; (c) the approaches to data analysis and related capabilities that have been developed for particle physics experiments will become increasingly important to CMB science as the scope of CMB experiments, and scale of the collaborations, increases. • Recommendations: PASAG recommends that QUIET II be supported at the proposed scope under all budget scenarios. Given the central importance of the CMB to our understanding of energy, matter, space, and time and the unique contributions HEP can provide to CMB science, PASAG further recommends that the future upgrade path for QUIET II should be considered for support at the appropriate time.” Field does support multiple efforts, e.g. Dark Matter searches FNAL PAC

  19. What Characterizes/Distinguishes QUIET? • Unique RF technology • Different systematics, Q & U measured simultaneously • Large dynamic range • Modulation: • 4 kHz inside modules • From sky rotation: Q to U to -Q every 6 hours • From telescope deck rotation: Q to U every week • ~6% of the sky mapped 100 times deeper than Planck • Sensitivity to r < 0.02 [based on current performance (noise, duty cycle)] • Alliance with (bolometric) POLARBEAR and ABS (and SPT) • Identical Patches • frequencies straddle WMAP “sweet spot” • HEP-like: • 800kHz digitization (FPGA demodulation) • Volume production, quality control • simulations, data reduction, blind analyses, systematics, systematics, ….. • Increased appreciation of our field • Upgrade Path: • Sharing ATACAMA telescopes • MMIC improvements: from 15 QL to 8 QL to 3QL FNAL PAC

  20. Bruce’s Backup Slides FNAL PAC

  21. ATACAMA Experiments 32/ NSF Site Visit – May 18 - 19, 2009 NSF Site Visit – May 18 - 19, 2009

  22. Lensing Simulation (W. Hu et al.) FNAL PAC

  23. Lensing BB Power Spectrum vs. Neutrino Mass FNAL PAC

  24. Current CMB Polarization Status (QUIET has already collected data which will improve these measurements) FNAL PAC

  25. Telescope • 1.4m primary mirror • FWHM: • 13 arcmin (W-band) • 28 arcmin (Q-band) FNAL PAC

  26. +Q -Q +Q -Q High Speed Sampling18 bits @ 800 kHz Q/U measurement every 250 s Monitors high-frequency noise Permits Quadrature Samples • TOD noise with no signal 0.5ms FNAL PAC

  27. Moon PRELIMINARY WMAP Galaxy (TT, <100 hrs) QUIET FNAL PAC

  28. CMB & Collider DM Constraints EPP2010 FNAL PAC

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